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Seasonal Variations in Airflow Over the Namib Dune, Gale Crater, Mars

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Seasonal Variations in Airflow Over the Namib Dune, Gale Crater, Mars Geophysical Research Letters RESEARCH LETTER Seasonal Variations in Airflow Over the Namib Dune, Gale 10.1029/2018GL079598 Crater, Mars: Implications for Dune Dynamics Key Points: Carin Cornwall1 , Derek W. T. Jackson1 , Mary C. Bourke2 , Meiring Beyers3, and • CFD data provide a more complete 1 understanding of Martian sediment J. Andrew G. Cooper transport, augmenting ripple 1 2 mapping studies Geography and Environmental Sciences, Ulster University, Coleraine, UK, Geography, Trinity College, Dublin, Ireland, 3 • Dune length scale modeling Klimaat Consulting, Guelph, Ontario, Canada highlights areas of elevated surface shear stress that affect localized sediment flux Abstract Dune length scale airflow modeling provides new insights on eolian bedform response and • Detailed seasonal 3-D airflow structures are presented that have complex near-surface 3-D wind patterns not previously resolved by mesoscale models. At a 1-m surface not been previously attainable using resolution, Curiosity wind data are used to investigate the eolian environment of the Namib dune on Mars, mesoscale models providing improved seasonal constraints on grainfall, grainflow activity, and ripple migration. Based on satellite images, airflow patterns, and surface shear stress, enhanced eolian activity, and slipface Supporting Information: advancement occurs during early springtime. Autumn and winter winds are also favorable to eolian activity, • Supporting Information S1 but minimal movement was detected in satellite images overlapping with wind data. During the summer, • Figure S1 • Figure S2 the migration of large stoss ripples on the Namib dune may augment sediment deposition on the slipface. • Figure S3 These results provide a better understanding of the overall migration pattern of the Namib dune, which • Figure S4 can be extrapolated to other dunes in the Bagnold Dune Field. • Figure S5 • Figure S6 Plain Language Summary At 1-m resolution, small-scale airflow modeling can provide new • Figure S7 • Figure S8 insights into sediment transport and dune migration on Mars. Coupled with wind data collected by the • Table S1 Curiosity rover, this study provides improved, realistic constraints on Martian sediment movement and illustrates how ripples seasonally form and migrate according to changing wind speeds and directions. The Correspondence to: spring season with northerly winds is the most influential for dune migration based on modeling results and C. Cornwall, [email protected] satellite monitoring, but the quieter summer and autumn seasons with southeasterly winds continue to facilitate ripple migration, which may help maintain slower rates of dune migration despite the opposing wind direction. Based on modeling results, the winter season with high-magnitude northerly winds should Citation: Cornwall, C., Jackson, D. W. T., Bourke, produce migration rates similar to spring, but according to satellite monitoring, dune migration stops. Small M. C., Beyers, M., & Cooper, J. A. G. amounts of frost in between sand grains on the dune surface may be responsible for this halt in dune (2018). Seasonal variations in airflow migration. These results can be applied to other dunes in the Bagnold Dune Field, which likely experience the over the Namib Dune, Gale Crater, Mars: Implications for dune dynamics. same seasonal patterns in sediment transport. Geophysical Research Letters, 45. https:// doi.org/10.1029/2018GL079598 1. Introduction Received 12 JUL 2018 fi Accepted 6 SEP 2018 Curiosity Rover provided the rst in situ observations and sediment analysis of Martian dunes while Accepted article online 11 SEP 2018 traversing the Bagnold Dune Field toward Aeolis Mons in Gale Crater (Figure S1). Images taken by Curiosity of the Namib dune slipface revealed a detailed record of grainflows, ripple formation, and tensional cracks (Cornwall, Bourke, et al., 2018; Ewing et al., 2017), similar to terrestrial dunes (Cornwall, Jackson, et al., 2018). The Bagnold dune field is active (Silvestro et al., 2013) but Curiosity visited the dunes during late autumn, a time of decreased eolian activity with little sediment movement (Bridges et al., 2017). The Martian atmospheric density and gravity are much lower than Earth, and therefore, wind speeds need to be 7 times greater to initiate grain saltation. However, once a grain is in motion, it can stay mobilized at a lower shear stress (Greeley et al., 1980; Greeley & Iversen, 1985; Kok, 2010a, 2010b; Kok et al., 2012; Kok & Renno, 2009). Based on terrestrial studies, grainflow formation requires an accumulation of sediment from grainfall, resulting in localized over-steepening, destabilization, and subsequent slope failure (e.g., Allen, 1970; Anderson, 1988; Hunter, 1985; McDonald & Anderson, 1995; Sutton et al., 2013). The preserved ©2018. The Authors. grainflows on the Namib dune slipface indicate that eolian conditions were favorable, at some point, to This is an open access article under the grainfall, but it is unclear precisely when grainfall occurred. terms of the Creative Commons Attribution License, which permits use, Airflow modeling research on Mars has focused largely on global patterns with general circulation models, distribution and reproduction in any which have provided a valuable foundation for understanding atmospheric-surface interactions (e.g., medium, provided the original work is properly cited. Fenton & Richardson, 2001; Greeley et al., 1993; Haberle et al., 1993; Hourdin & Forget, 1995; Leovy & CORNWALL ET AL. 1 Geophysical Research Letters 10.1029/2018GL079598 Mintz, 1969; Lee & Thomas, 1995; Richardson et al., 2007). However, dunes are heavily influenced by local wind patterns, unresolved by general circulation models, that shape morphology and control sediment trans- port (e.g., Fenton et al., 2005; Greeley et al., 1993, 2006; Hayward et al., 2007, 2008, 2009). Mesoscale climate models, with a resolution of hundreds of meters, have achieved a more detailed study of local wind regimes, providing a regional context of short-timescale wind flow variability but are better suited for dune field airflow analysis (e.g., Fenton et al., 2005; Hobbs et al., 2010; Newman et al., 2017; Pla-Garcia et al., 2016; Rafkin et al., 2001, 2016; Richardson et al., 2007; Spiga & Forget, 2009; Toigo & Richardson, 2002; Tyler et al., 2002). Mesoscale models with bedform morphology analysis of the Bagnold Dune Field revealed a bimodal wind regime influenced by the crater floor topography with primary winds from the NW and secondary winds from the NE (Bridges et al., 2017; Day & Kocurek, 2016; Hobbs et al., 2010; Newman et al., 2017; Silvestro et al., 2013, 2016). Unfortunately, with model resolutions of ~500 m, forcing mechanisms that drive dune migration cannot be studied in full detail (Newman et al., 2017; Pla-Garcia et al., 2016; Rafkin et al., 2016), preventing a more comprehensive understanding of eolian processes operat- ing in Gale Crater. Analysis of eolian morphodynamics of individual dunes requires a spatial scale smaller than the dimensions of the dune to properly assess how local wind patterns affect eolian processes. Local topography can signifi- cantly influence wind speed and direction, thereby also affecting surface shear stress and enabling sediment transport during seasons of low magnitude winds. Eolian 2-D ripple mapping studies can offer some insights into surface airflow and sediment flux, but in areas absent of ripples, there is no information on airflow direc- tion or magnitude modification, which can significantly impact dune morphology and create localized areas of greater surface shear stress. In addition, knowledge of detailed 3-D flow structures and turbulence is unat- tainable using mesoscale models or ripple mapping techniques. Recent efforts have employed 3-D dune length scale computational fluid dynamics (CFD) modeling with a resolution <5 m to investigate these smaller airflow patterns and how they influence dune morphology and sediment transport (Jackson et al., 2015). This study uses a dune length scale CFD model with a High Resolution Imaging Science Experiment (HiRISE) Digital Terrain Model (DTM) of the Namib dune at a 1-m horizontal resolution, which adequately resolves subdune scale bedforms and provides a more com- prehensive investigation of complex airflow patterns (Jackson et al., 2015). Seasonal results of dune length scale airflow modeling reveal complex, turbulent, and steered airflow on the dune slipface as well as in the immediate vicinity of the dune. An investigation of how these complex seasonal flow patterns may affect grainflow activity on the slipface and overall dune migration is presented for the Namib dune (À4.686°N, 222.364°W) using Mars Science Laboratory’s (MSL) Curiosity Rover Environmental Monitoring Station (REMS) data (S2), a HiRISE DEM (S3), and the open source CFD software OpenFOAM (S4) to simulate the local Martian wind regime. 2. Results The local wind regime in Gale Crater is complex, with a wide range of wind directions and magnitudes during a single Mars year (MY; Figure S1). REMS data in this study include MY 32 summer and MY 33 autumn, winter, and spring and indicates that the greatest magnitude near-surface winds predominantly originated from the north, agreeing with dune orientation and migration to the south. Lesser magnitude winds also occurred, and it appears that southerly winds may also have an impact on dune morphology and slipface processes. 2.1. Seasonal Patterns 2.1.1. Spring (Ls 180°) Higher magnitude winds occurred early in the season, between Martian solar days ~1,400 and 1,430 and ori- ginated from the north (Figure 1) with an average wind velocity of 9.84 m/s (Table S4). The more predominant but lesser magnitude winds during the spring varied between east, southeast, and southwest (Figure 1). These secondary winds had an average wind speed of 7.70 m/s (Table S4). High amounts of surface shear stress were present in most areas of the stoss slope during primary winds and À À greatest along the dune brink with a maximum value of 0.027 kg · m 1 ·s 2 with near-surface winds reaching approximately 17 m/s (Figures 2 and S6). Significant turbulent flow was generated on the lee side of the CORNWALL ET AL.
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